The Einstein equations alone do not enforce any particular signature. For example, in the derivation of the Schwarzschild metric you require that the metric is asymptotically flat... but not just any flat metric: by doing so you typically require that it's the flat Minkowski metric, not the flat Euclidean one. However, you may do the same by requiring that the metric is asymptotically Euclidean! While this is mathematically possible, this wouldn't be a GR solution: if you are doing GR you have to implement a Minkowsky-like metric in the boundary conditions.
Therefore, the signature is cooked into the boundary conditions or in the initial value if you have a Cauchy problem. It is so because having a Lorentzian signature is a fundamental requirement of GR (it is fundamental for the causal structure). However, this is something that should be explicitly implemented when solving the Einstein equations. Since the Einstein equations are partial differential equations, information on the signature enters via the initial condition or boundary terms (depending on the practical problem at hand).
As a final note, a common way of implementing the Lorentzian nature in a practical way is to rely on the 3+1 split of spacetime for solving the Cauchy initial value problem but, again, this is not strictly necessary and you must have an initial condition consistent with a Lorentzian metric.