  We derive effective equations with loop quantum gravity corrections for the
Lema\^itre-Tolman-Bondi family of space-times, and use these to study quantum
gravity effects in the Oppenheimer-Snyder collapse model. For this model, after
the formation of a black hole with an apparent horizon, quantum gravity effects
become important in the space-time region where the energy density and
space-time curvature scalars become comparable to the Planck scale. These
quantum gravity effects first stop the collapse of the dust matter field when
its energy density reaches the Planck scale, and then cause the dust field to
begin slowly expanding. Due to this continued expansion, the matter field will
eventually extend beyond the apparent horizon, at which point the horizon
disappears and there is no longer a black hole. There are no singularities
anywhere in this space-time. In addition, in the limit that edge effects are
neglected, we show that the dynamics for the interior of the star of uniform
energy density follow the loop quantum cosmology effective Friedman equation
for the spatially flat Friedman-Lema\^itre-Robertson-Walker space-time.
Finally, we estimate the lifetime of the black hole, as measured by a distant
observer, to be $\sim (GM)^2/\ell_{\rm Pl}$.
