  Dissipationless collapses in Modified Newtonian Dynamics (MOND) are studied
by using a new particle-mesh N-body code based on our numerical MOND potential
solver. We found that low surface-density end-products have shallower inner
density profile, flatter radial velocity-dispersion profile, and more radially
anisotropic orbital distribution than high surface-density end-products. The
projected density profiles of the final virialized systems are well described
by Sersic profiles with index m~4, down to m~2 for a deep-MOND collapse.
Consistently with observations of elliptical galaxies, the MOND end-products,
if interpreted in the context of Newtonian gravity, would appear to have little
or no dark matter within the effective radius. However, we found impossible
(under the assumption of constant mass-to-light ratio) to simultaneously place
the resulting systems on the observed Kormendy, Faber-Jackson and Fundamental
Plane relations of elliptical galaxies. Finally, the simulations provide strong
evidence that phase mixing is less effective in MOND than in Newtonian gravity.
