This question is based on page 68 of Thomas Hartman's notes on Quantum Gravity and Black Holes.
To evaluate a path integral in ordinary quantum field theory, we integrate over fields defined on a fixed spacetime manifold.
In quantum gravity, however, we integrate over both the (non-gravitational) fields and the geometry. The (Euclidean) gravitational path integral is therefore
$$\int \mathcal{D}g\mathcal{D}\phi\ e^{-S_{E}[g,\phi]},$$
with the boundary conditions
$$t_{E} \sim t_{E} + \beta, \qquad g_{tt} \to 1\ \text{as}\ r \to \infty.$$
How would you explain these boundary conditions without alluding to finite-temperature quantum field theory?