  We use the public code ebhlight to carry out 3D radiative general
relativistic magnetohydrodynamics (GRMHD) simulations of accretion onto the
supermassive black hole in M87. The simulations self-consistently evolve a
frequency-dependent Monte Carlo description of the radiation field produced by
the accretion flow. We explore two limits of accumulated magnetic flux at the
black hole (SANE and MAD), each coupled to several sub-grid prescriptions for
electron heating that are motivated by models of turbulence and magnetic
reconnection. We present convergence studies for the radiation field and study
its properties. We find that the near-horizon photon energy density is an order
of magnitude higher than is predicted by simple isotropic estimates from the
observed luminosity. The radially dependent photon momentum distribution is
anisotropic and can be modeled by a set of point-sources near the equatorial
plane. We draw properties of the radiation and magnetic field from the
simulation and feed them into an analytic model of gap acceleration to estimate
the very high energy (VHE) gamma-ray luminosity from the magnetized jet funnel,
assuming that a gap is able to form. We find luminosities of $\rm \sim 10^{41}
\, erg \, s^{-1}$ for MAD models and $\rm \sim 2\times 10^{40} \, erg \,
s^{-1}$ for SANE models, which are comparable to measurements of M87's VHE
flares. The time-dependence seen in our calculations is insufficient to explain
the flaring behavior. Our results provide a step towards bridging theoretical
models of near-horizon properties seen in black hole images with the VHE
activity of M87.
