  We conclude the study of the Post-Minkowskian linearization of ADM tetrad
gravity in the York canonical basis for asymptotically Minkowskian space-times
in the family of non-harmonic 3-orthogonal gauges parametrized by the York time
${}^3K(\tau, \vec \sigma)$ (the inertial gauge variable, not existing in Newton
gravity, describing the general relativistic remnant of the freedom in clock
synchronization in the definition of the instantaneous 3-spaces). As matter we
consider only N scalar point particles with a Grassmann regularization of the
self-energies and with a ultraviolet cutoff making possible the PM
linearization and the evaluation of the PM solution for the gravitational
field. We study in detail all the properties of these PM space-times
emphasizing their dependence on the gauge variable ${}^3{\cal K}_{(1)} =
{1\over {\triangle}}\, {}^3K_{(1)}$ (the non-local York time): Riemann and Weyl
tensors, 3-spaces, time-like and null geodesics, red-shift and luminosity
distance. Then we study the Post-Newtonian (PN) expansion of the PM equations
of motion of the particles. We find that in the two-body case at the 0.5PN
order there is a damping (or anti-damping) term depending only on ${}^3{\cal
K}_{(1)}$. This open the possibility to explain dark matter in Einstein theory
as a relativistic inertial effect: the determination of ${}^3{\cal K}_{(1)}$
from the masses and rotation curves of galaxies would give information on how
to find a PM extension of the existing PN Celestial frame (ICRS) used as
observational convention in the 4-dimensional description of stars and
galaxies. Dark matter would describe the difference between the inertial and
gravitational masses seen in the non-Euclidean 3-spaces, without a violation of
their equality in the 4-dimensional space-time as required by the equivalence
principle.
