How do we measure the velocity in curved space-time? In almost general case, the space-time metrics looks like:
\begin{equation}
 ds^2 = g_{00}(dx^0)^2 + 2g_{0i}dx^0dx^i + g_{ik}dx^idx^k,
\end{equation}
where $i,k = 1 \ldots 3$ - are spatial indeces.
The spatial distance between points (as determined, for example, by the stationary observer):
\begin{equation}
 dl^2 = \left( -g_{ik} + \frac{g_{0i}g_{0j}}{g_{00}}\right)dx^idx^j = \gamma_{ik}dx^idx^j,
\end{equation}
where
\begin{equation}
 \gamma_{ik} = -g_{ik} + \frac{g_{0i}g_{0j}}{g_{00}} ,
\end{equation}
And we can rewrite merics in a form:
\begin{equation}
 ds^2 = g_{00}(dx^0 - g_idx^i)^2 - dl^2,
\end{equation}
in the last expression $g_i$ is:
\begin{equation}\label{vecg}
 g_i = -\frac{g_{0i}}{g_{00}}.
\end{equation}
My question in general souns like, how do the velocity of a certain particle are determined by different types of observers?
Or special case: which type of the observer can determine velocity $v^2 = \frac{dl^2}{g_{00}(dx^0 - g_idx^i)^2}$? 
I am confused by the fact that time $\sqrt{g_{00}}(dx^0 - g_idx^i)$ is not the proper time of any observer. What is this time?
I had draw the space-time diagram to clarify my question. Here $x^0$ - coordinate time, $t$ - "orthogonal" time defined as $dt = dx^0 - g_idx^i$. Is it correct?

 A: I assume that, referring to local coordinates $x^0,x^1,x^2,x^3$, the vector  $\partial_{x^0}$ is timelike and $\partial_{x^i}$ are spacelike for $i=1,2,3$.
I henceforth use the signature $-,+,+,+$.
Notions like velocity can be defined in general coordinate systems but some precautions  are necessary. 


*

*First of all $x^0$ is not the physical time measured along timelike curves $x^i=$ constant (i=1,2,3) representing observers at rest with the coordinates and thus parametrized by the coordinate $x^0$. The physical time, measured with physical clocks, is the proper time along these curves $d\tau = \sqrt{-g_{00}} dx^0$. In practical terms, a "small" displacement $$\Delta a \partial_{x^0}$$ along this temporal axis corresponds to a physical interval of time 
$$\Delta\tau = \sqrt{-g(\Delta a \partial_{x^0},\Delta a \partial_{x^0})}= \Delta a \sqrt{-g_{00}}$$    

*A spacelike $3$-surface $\Sigma_{x^0}$  defined by fixing  $x^0=$ constant can be interpreted as the rest space of the coordinate system provided a suitable (Euclidean) metric is defined on it. This is not the usual metric $h$ induced by $g$ in the standard way $h(X,Y):= g(X,Y)$ for $X,Y$ tangent to $\Sigma_{x^0}$. The definition of the physically correct metric arises form the constraint that light-like paths must have constant velocity $1$. 
It is not difficult to prove that (e.g., see Landau-Lifsits' book on Field Theory sect. 84 ch.10 for a nice physical "proof") the appropriate metric is just that you wrote.
If you consider a pair of vectors tangent to the rest space $\Sigma_{x^0}$, i.e.,
$$X= \sum_{i=1}^3 X^i\partial_{x^i}\quad \mbox{and} \quad Y= \sum_{i=1}^3 Y^i\partial_{x^i}$$
then the physical scalar product is
$$\gamma(X,Y) := \sum_{i,j=1}^3 \left(g_{ij} - \frac{g_{i0}g_{j0}}{g_{00}}\right) X^iY^j\:.$$
Notice that $\gamma$ is defined on all vectors in spacetime not only those tangent to $\Sigma_{x^0}$:
If $$X=  X^\mu\partial_{x^\mu}\quad \mbox{and} \quad Y=  Y^\nu\partial_{x^\nu}$$
$$\gamma(X,Y) := \left(g_{\mu\nu} - \frac{g_{\mu 0}g_{\nu 0}}{g_{00}}\right) X^\mu Y^\nu =  \sum_{i,j=1}^3 \left(g_{ij} - \frac{g_{i0}g_{j0}}{g_{00}}\right) X^iY^j$$
and it automatically extracts the spatial part of them, since $\gamma(X, \partial_{x^0})=0$.
Now we pass to the definition of velocity of a particle with respect to the said reference frame. The story of the particle is a curve $x^\mu = x^\mu(s)$, the nature of $s$ does not matter. The tangent vector to this curve is $$X= \frac{dx^\mu}{ds} \partial_{x^\mu}$$
We can write, if the curve is sufficiently smooth, 
$$x^\mu(s+ \Delta s) = x^\mu(s) + \Delta s X^\mu(s) + O((\Delta s^2)) \:.$$
During the interval of parameter $\Delta s$, the particle runs in $\Sigma_{x^{0}(s)}$ an amount of  physical space
$$\Delta l = \sqrt{\gamma\left( \Delta s X,\Delta s X\right)} = \Delta s \sqrt{\gamma(X,X)}$$
up to second order $\Delta s$ infinitesimals.
The corresponding amount of physical time is extracted from the orthogonal projection of $\Delta s X$ along the time axis $\partial_{x^0}$ taking its normalization into account:
 $$T = g\left( \Delta s X, \frac{\partial_{x^0}}{\sqrt{-g_{00}}}\right) \frac{\partial_{x^0}}{\sqrt{-g_{00}}} = \Delta s \frac{X^0 g_{00} + \sum_{i=1}^3 g_{0i}X^i}{-g_{00}}\partial_{x^0}\:.$$ 
According to my first comment above, the length (with respect to $g$) of this vector is just the amount of physical time spent by the particle in the interval $\Delta s$ of parameter. This time is measured by the proper time of a clock moving along the $x^0$ axis. 
$$\Delta \tau = \sqrt{-g(T,T)} = \Delta s \frac{X^0 g_{00} + \sum_{i=1}^3 g_{0i}X^i}{\sqrt{-g_{00}}}$$
up to second order $\Delta s$ infinitesimals.  
In summary, the velocity of the particle referred to the coordinates $x^0,x^1,x^2,x^3$ is 
$$v = \lim_{\Delta s \to 0}\frac{\Delta l}{\Delta \tau} = \sqrt{-g_{00}}\frac{\sqrt{\gamma(X,X)}}{X^0 g_{00} + \sum_{i=1}^3 g_{0i}X^i}$$ so that
$$v^2 = -g_{00}\frac{\gamma(X,X)}{(X^0 g_{00} + \sum_{i=1}^3 g_{0i}X^i)^2} $$
This is the rigorous expression of the formula you wrote. The vector $X$ in your case has components $X^\mu = dx^\mu$. The minus sign in front of the right-hand side is just due to the different choice of the signature of the metric. 
COMMENT. These notions are not related with the choice of a curved spacetime. Everything is valid also in Minkowski spacetime referring to non-Minkowskian coordinates with $g_{0k}\neq 0$ (and possibly $g_{00} \neq -1$). A standard example are coordinates at rest with a rotating platform with respect to an inertial system in Minkowki spacetime.
A: You write

The spatial distance between points (as determined, for example, by
  the stationary observer)...

But don't forget spatial distance is relative to the observer; recall "length-contraction" as taught in introductory special relativity. It is only those observers which are comoving with your given coordinate system $x^\mu$ which determine your spatial metric $\gamma_{ik}$. These observers have 4-velocity $(1/\sqrt{g_{00}},0,0,0)$, under your +--- metric signature. The spatial metric you give was derived by Landau & Lifshitz in their fields textbook (see $\S84$ in the 1994 edition). Landau & Lifshitz do state this assumption of comoving observers, and also give conditions for when such observers exist. Different observers will determine a different spatial 3-metric. I am writing a paper on such topics, and will link it when completed.
The discussed properties should be understood as only local, meaning in the immediate vicinity of the observer; this is particularly true in curved spacetime.
As for relative velocity in curved spacetime, suppose $\mathbf u$ and $\mathbf v$ are two observers (4-velocities) at the same event. Then their relative 3-velocity has Lorentz factor
$$\gamma=\mathbf u\cdot\mathbf v$$
assuming metric signature +---. See Carroll's textbook.
