  We present ALMA 1.3 mm continuum, 12CO, C18O, and SO data for the Class 0
protostars, Lupus 3 MMS, IRAS 15398-3559, and IRAS 16253-2429 at resolutions of
~100 AU. By measuring a rotational profile in C18O, a 100 AU Keplerian disk
around a 0.3 Msun protostar is observed in Lupus 3 MMS. No 100 AU Keplerian
disks are observed in IRAS 15398-3559 and IRAS 16253-2429. Nevertheless,
embedded compact (<30 AU) continuum components are detected. The C18O emission
in IRAS 15398-3559 shows signatures of infall with a constant angular momentum.
IRAS 16253-2429 exhibits signatures of infall and rotation, but its rotational
profile is unresolved. By fitting the C18O data with our kinematic models, the
protostellar masses and the disk radii are inferred to be 0.01 Msun and 20 AU
in IRAS 15398-3559, and 0.03 Msun and 6 AU in IRAS 16253-2429. By comparing the
specific angular momentum profiles from 10,000 to 100 AU in 8 Class 0 and I
protostars, we find that the evolution of envelope rotation can be described
with conventional inside-out collapse models. In comparison with a sample of 18
protostars with known disk radii, our results reveal signs of disk growth, with
the disk radius increasing as M*^{0.8+/-0.14} or t^{1.09+\-0.37} in the Class 0
stage, where M* is the protostellar mass and t is the age. The disk growth rate
slows down in the Class I stage. Besides, we find a hint that the mass
accretion rate declines as t^{-0.26+\-0.04} from the Class 0 to I stages.
