  We present 3D general relativistic magnetohydrodynamic (GRMHD) simulations of
the accretion flow surrounding Sagittarius A* that are initialized using
larger-scale MHD simulations of the $\sim$ 30 Wolf--Rayet (WR) stellar winds in
the Galactic center. The properties of the resulting accretion flow on horizon
scales are set not by ad hoc initial conditions but by the observationally
constrained properties of the WR winds with limited free parameters. For this
initial study we assume a non-spinning black hole. Our simulations naturally
produce a $\sim 10^{-8} M_\odot$ yr$^{-1}$ accretion rate, consistent with
previous phenomenological estimates. We find that a magnetically arrested flow
is formed by the continuous accretion of coherent magnetic field being fed from
large radii. Near the event horizon, the magnetic field is so strong that it
tilts the gas with respect to the initial angular momentum and concentrates the
originally quasi-spherical flow to a narrow disk-like structure. We also
present 230 GHz images calculated from our simulations where the inclination
angle and physical accretion rate are not free parameters but are determined by
the properties of the WR stellar winds. The image morphology is highly time
variable. Linear polarization on horizon scales is coherent with weak internal
Faraday rotation.
