  In this paper, we present the results of our three-dimensional, multi-group,
multi-neutrino-species radiation/hydrodynamic simulation using the
state-of-the-art code F{\sc{ornax}} of the terminal dynamics of the core of a
non-rotating 16-M$_{\odot}$ stellar progenitor. The calculation incorporates
redistribution by inelastic scattering, a correction for the effect of
many-body interactions on the neutrino-nucleon scattering rates, approximate
general relativity (including the effects of gravitational redshifts),
velocity-dependent frequency advection, and an implementation of initial
perturbations in the progenitor core. The model explodes within $\sim$100
milliseconds of bounce (near when the silicon-oxygen interface is accreted
through the temporarily-stalled shock) and by the end of the simulation (here,
$\sim$677 milliseconds after bounce) is accumulating explosion energy at a rate
of $\sim$2.5$\times$10$^{50}$ ergs s$^{-1}$. The supernova explosion resembles
an asymmetrical multi-plume structure, with one hemisphere predominating. The
gravitational mass of the residual proto-neutron star at $\sim$677 milliseconds
is $\sim$1.42 M$_{\odot}$. Even at the end of the simulation, explosion in most
of the solid angle is accompanied by some accretion in an annular fraction at
the wasp-like waist of the debris field. The ejecta electron fraction (Y$_e$)
is distributed from $\sim$0.48 to $\sim$0.56, with most of the ejecta mass
proton-rich. This may have implications for supernova nucleosynthesis, and
could have a bearing on the p- and $\nu$p-processes and on the site of the
first peak of the r-process. The ejecta spatial distributions of both Y$_e$ and
mass density are predominantly in wide-angle plumes and large-scale structures,
but are nevertheless quite patchy.
