  Structure formation in young protoplanetary disks is investigated using a
one-dimensional model including the formation and the evolution of disks.
Recent observations with ALMA found that a ring-hole structure may be formed in
young protoplanetary disks, even when the disk is embedded in the envelope. We
present a one-dimensional model for the formation of a protoplanetary disk from
a molecular cloud core and its subsequent long-term evolution within a single
framework. Such long-term evolution has not been explored by numerical
simulations due to the limitation of computational power. In our model, we
calculate the time evolution of the surface density of the gas and the dust
with the wind mass loss and the radial drift of the dust in the disk. We find
that the MHD disk wind is a viable mechanism for the formation of ring-hole
structure in young disks. We perform a parameter study of our model and derive
condition of the formation of ring-hole structures within $6\times10^5$ years
after the start of the collapse of the molecular cloud core. The final outcome
of the disk shows five types of morphology and this can be understood by
comparing the timescale of the viscous diffusion, the mass loss by MHD disk
wind and the radial drift of the dust. We discuss the implication of the model
for the WL 17 system, which is suspected to be an embedded, yet transitional,
disk.
