We present axisymmetric two-temperature general relativistic radiation magnetohydrodynamic ( GRRMHD ) simulations of the inner region of the accretion flow onto the supermassive black hole M87 . We address uncertainties from previous modeling efforts through inclusion of models for ( 1 ) self-consistent dissipative and Coulomb electron heating ( 2 ) radiation transport ( 3 ) frequency-dependent synchrotron emission , self-absorption , and Compton scattering . We adopt a distance D = 16.7 Mpc , an observer angle \theta = 20 \degree , and consider black hole masses M / M _ { \odot } = ( 3.3 \times 10 ^ { 9 } , 6.2 \times 10 ^ { 9 } ) and spins a _ { \star } = ( 0.5 , 0.9375 ) in a four-simulation suite . For each ( M,a _ { \star } ) , we identify the accretion rate that recovers the 230 GHz flux from very long baseline interferometry measurements . We report on disk thermodynamics at these accretion rates ( \dot { M } / \dot { M } _ { \mathrm { Edd } } \sim 10 ^ { -5 } ) . The disk remains geometrically thick ; cooling does not lead to a thin disk component . While electron heating is dominated by Coulomb rather than dissipation for r \gtrsim 10 GM / c ^ { 2 } , the accretion disk remains two-temperature . Radiative cooling of electrons is not negligible , especially for r \lesssim 10 GM / c ^ { 2 } . The Compton y parameter is of order unity . We then compare derived and observed or inferred spectra , millimeter images , and jet powers . Simulations with M / M _ { \odot } = 3.3 \times 10 ^ { 9 } are in conflict with observations . These simulations produce millimeter images that are too small , while the low-spin simulation also overproduces X-rays . For M / M _ { \odot } = 6.2 \times 10 ^ { 9 } , both simulations agree with constraints on radio/IR/X-ray fluxes and millimeter image sizes . Simulation jet power is a factor 10 ^ { 2 } -10 ^ { 3 } below inferred values , a possible consequence of the modest net magnetic flux in our models .