  The Event Horizon Telescope mass estimate for M87* is consistent with the
stellar dynamics mass estimate, and inconsistent with the gas dynamics mass
estimates by up to $2\sigma$. We have previously explored a new gas dynamics
model that incorporated sub-Keplerian gas velocities that could in principle
explain the discrepancy in the stellar and gas dynamics mass estimate. In this
paper, we extend this gas dynamical model to also include non-trivial disk
heights, which may also resolve the mass discrepancy independent of
sub-Keplerian velocity components. By combining the existing velocity
measurements and the EHT mass estimate, we place constraints on the gas disk
inclination and sub-Kelplerian fraction. These constraints require the
parsec-scale ionized gas disk be misaligned with the milli-arcsecond radio jet
by at least $11^{\circ}$, and more typically $27^{\circ}$. Modifications to the
gas dynamics model either by introducing sub-Keplerian velocities or thick
disks produces further misalignment with the radio jet. If the jet is produced
in a Blandford-Znajek-type process, the angular momentum of the black hole is
decoupled with the angular momentum of the large scale gas feeding M87*.
