  In a previous work we derived an effective Hamiltonian constraint for the
Schwarzschild geometry starting from the full loop quantum gravity Hamiltonian
constraint and computing its expectation value on coherent states sharply
peaked around a spherically symmetric geometry. We now use this effective
Hamiltonian to study the interior region of a Schwarzschild black hole, where a
homogeneous foliation is available. Descending from the full theory, our
effective Hamiltonian, though still bearing the well known ambiguities of the
quantum Hamiltonian operator, preserves all relevant information about the
fundamental discreteness of quantum space. This allows us to have a uniform
treatment for all quantum gravity holonomy corrections to spatially homogeneous
geometries, unlike the minisuperspace loop quantization models in which the
effective Hamiltonian is postulated. We show how, for several geometrically and
physically well motivated choices of coherent states, the classical black hole
singularity is replaced by a homogeneous expanding Universe. The resultant
geometries have no significant deviations from the classical Schwarzschild
geometry in the pre-bounce sub-Planckian curvature regime, evidencing the fact
that large quantum effects are avoided in these models. In all cases, we find
no evidence of a white hole horizon formation. However, various aspects of the
post-bounce effective geometry depend on the choice of quantum states.
