  In our previous study (Tsukamoto {\it et al.} 2023), we investigated
formation and early evolution of protoplanetary disks with 3D non-ideal
magnetohydrodynamics simulations considering dust growth, and found that the
modified equations of the conventional steady accretion disk model which
consider the magnetic braking, { dust growth} and ambipolar diffusion reproduce
the disk structure obtained from simulations very well. In this paper, as a
sequel of the our previous study, we analytically investigate the structure and
evolution of protoplanetary disks corresponding to Class 0/I young stellar
objects using the modified steady accretion disk model combining an analytical
model of envelope accretion. We estimate that the disk radius is several AU at
disk formation epoch and increases to several 100 AU at the end of the
accretion phase. The disk mass is estimated to be $0.01 M_\odot \lesssim M_{\rm
disk} \lesssim 0.1 M_\odot$ for a disk with radius of several 10 AU and mass
accretion rate of $\dot{M}_{\rm disk} \sim 10^{-6} M_\odot {\rm yr^{-1}}$. We
also found that, with typical disk ionization rates and moderate mass accretion
rate ($\dot{M}_{\rm disk}\gtrsim10^{-8} M_\odot {\rm yr^{-1}}$),
magneto-rotational instability is suppressed in the disk because of low plasma
$\beta$ and efficient ambipolar diffusion. We argue that the radial profile of
specific angular momentum (or rotational velocity) at the disk outer edge
should be continuously connected to that of the envelope if the disk evolves by
magnetic braking, and should be discontinuous if the disk evolves by internal
angular momentum transport process such as gravitational instability or
magneto-rotational instability. Future detailed observations of the specific
angular momentum profile around the disk outer edge are important for
understanding the angular momentum transport mechanism of protoplanetary disks.
