  We investigate both the classical and quantum gravitational collapse of a
charged, non-rotating $n$-dimensional BTZ black hole in AdS space. This is done
by first deriving the conserved mass of a "spherically" symmetric domain wall,
which is then taken as the classical Hamiltonian of the domain wall.
  In the classical picture, we show that, as far as the asymptotic observer is
concerned, the details of the collapse depend on the amount of charge present
in the domain wall. In the both the extremal and non-extremal cases, the
collapse takes an infinite amount of observer time to complete. However, in the
over-charged case, the collapse never actually occurs, instead one finds an
oscillatory solution which prevents the formation of a naked singularity. As
far as the infalling observer is concerned, the collapse is completed within a
finite amount of proper time. Thus, the gravitational collapse follows that of
the typical formation of a black hole via gravitational collapse.
  Quantum mechanically, in the absence of induced quasi-particle production and
fluctuations of the metric geometry, we take primary interest in the behavior
of the collapse near the horizon and near the classical singularity from the
point of view of both asymptotic and infalling observers. For the asymptotic
observer, we find that quantum effects near the horizon do not change the
classical conclusions. For the infalling observer, the most interesting quantum
mechanical effect are when the collapsing shell approaches the classical
singularity. Here, we find, that the quantum effects in this region display
non-local effects, which depend on the energy density of the domain wall.
