  We run three long-timescale general-relativistic magnetohydrodynamic
simulations of radiatively inefficient accretion flows onto non-rotating black
holes. Our aim is to achieve steady-state behavior out to large radii and
understand the resulting flow structure. A simulation with adiabatic index
Gamma = 4/3 and small initial alternating poloidal magnetic field loops is run
to a time of 440,000 GM/c^3, reaching inflow equilibrium inside a radius of 370
GM/c^2. Variations with larger alternating field loops and with Gamma = 5/3 are
run to 220,000 GM/c^3, attaining equilibrium out to 170 GM/c^2 and 440 GM/c^2.
There is no universal self-similar behavior obtained at radii in inflow
equilibrium: the Gamma = 5/3 simulation shows a radial density profile with
power law index ranging from -1 in the inner regions to -1/2 in the outer
regions, while the others have a power-law slope ranging from -1/2 to close to
-2. Both simulations with small field loops reach a state with polar inflow of
matter, while the more ordered initial field has polar outflows. However,
unbound outflows remove only a factor of order unity of the inflowing material
over a factor of ~300 in radius. Our results suggest that the dynamics of
radiatively inefficient accretion flows are sensitive to how the flow is fed
from larger radii, and may differ appreciably in different astrophysical
systems. Millimeter images appropriate for Sgr A* are qualitatively (but not
quantitatively) similar in all simulations, with a prominent asymmetric image
due to Doppler boosting.
