  We apply standard disk formation theory with adiabatic contraction within
cuspy halo models predicted by the standard LCDM cosmology. The resulting
models score remarkably well when confronted with the broad range of
observational data available for the Milky Way and M31 galaxies, giving a Milky
Way virial mass of 1-2x10^12Msun and concentration C=12-17. We consider two
types of models, in which: (A) baryons conserve angular momentum and (B) some
of the angular momentum of the baryons is transferred to the dark matter.
Type-A models produce good agreement with observed rotation curves and obey
constraints in the solar neighborhood, but may have too much dark matter in the
center to allow a fast rotating bar. The type-B models with angular momentum
transport have a slightly more massive disk and less dark matter in the central
part, allowing a fast rotating bar to persist. Both classes of models probably
have sufficient baryonic mass in the central 3.5kpc to reproduce recent
observational values of the optical depth to microlensing events towards the
Galactic center. All models require that about 1/2 of all baryons expected
inside the virial radius must not be in the disk or bulge. We investigate
whether the range of virial masses allowed by our dynamical models is
compatible with constraints from the galaxy luminosity function, and find a
range of parameter space that is allowed by this constraint. We conclude that
rotation curves and dynamical properties of ``normal'' high surface brightness
spiral galaxies appear to be consistent with standard LCDM.
