  We analyze three-dimensional magnetohydrodynamic (MHD) simulations of a
nonradiative accretion flow around a black hole using a pseudo-Newtonian
potential. The flow originates from a torus initially centered at 100
gravitational (Schwarzschild) radii. Accretion is driven by turbulent stresses
generated self-consistently by the magnetorotational instability. The resulting
flow has three well-defined dynamical components: a hot, thick,
rotationally-dominated Keplerian disk; a surrounding magnetized corona with
vigorous circulation and outflow; and a magnetically-confined jet along the
centrifugal funnel wall. Inside of 10 gravitational radii, the disk becomes
very hot, more toroidal, and highly intermittent. These results contrast
sharply with quasi-spherical, self-similar viscous models. There are no
significant dynamical differences between simulations that include resistive
heating and those that do not. We conclude by deducing some simple radiative
properties of our solutions, and apply the results to the accretion-powered
Galactic center source Sgr A*.
