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We conclude the study of the Post-Minkowskian linearization of ADM tetradgravity in the York canonical basis for asymptotically Minkowskian space-timesin the family of non-harmonic 3-orthogonal gauges parametrized by the York time${}^3K(\tau, \vec \sigma)$ (the inertial gauge variable, not existing in Newtongravity, describing the general relativistic remnant of the freedom in clocksynchronization in the definition of the instantaneous 3-spaces). As matter weconsider only N scalar point particles with a Grassmann regularization of theself-energies and with a ultraviolet cutoff making possible the PMlinearization and the evaluation of the PM solution for the gravitationalfield. We study in detail all the properties of these PM space-timesemphasizing their dependence on the gauge variable ${}^3{\cal K}_{(1)} ={1\over {\triangle}}\, {}^3K_{(1)}$ (the non-local York time): Riemann and Weyltensors, 3-spaces, time-like and null geodesics, red-shift and luminositydistance. Then we study the Post-Newtonian (PN) expansion of the PM equationsof motion of the particles. We find that in the two-body case at the 0.5PNorder there is a damping (or anti-damping) term depending only on ${}^3{\calK}_{(1)}$. This open the possibility to explain dark matter in Einstein theoryas a relativistic inertial effect: the determination of ${}^3{\cal K}_{(1)}$from the masses and rotation curves of galaxies would give information on howto find a PM extension of the existing PN Celestial frame (ICRS) used asobservational convention in the 4-dimensional description of stars andgalaxies. Dark matter would describe the difference between the inertial andgravitational masses seen in the non-Euclidean 3-spaces, without a violation oftheir equality in the 4-dimensional space-time as required by the equivalenceprinciple.

The Einstein-Maxwell-Particle System in the York Canonical Basis of ADM  Tetrad Gravity: III) The Post-Minkowskian N-Body Problem, its Post-Newtonian  Limit in Non-Harmonic 3-Orthogonal Gauges and Dark Matter as an Inertial  Effect