  Fragmentation process in a cylindrical magnetized cloud is studied with the
nested grid method. The nested grid scheme use 15 levels of grids with
different spatial resolution overlaid subsequently, which enables us to trace
the evolution from the molecular cloud density $\sim 100 {\rm cm}^{-3}$ to that
of the protostellar disk $\sim 10^{10} {\rm cm} ^{-3}$ or more. Fluctuation
with small amplitude grows by the gravita- tional instability. It forms a disk
perpendicular to the magnetic fields which runs in the direction parallel to
the major axis of the cloud. Matter accrets on to the disk mainly flowing along
the magnetic fields and this makes the column density increase. The radial
inflow, whose velocity is slower than that perpendicular to the disk, is driven
by the increase of the gravity. While the equation of state is isothermal and
magnetic fields are perfectly coupled with the matter, which is realized in the
density range of $\rho \lesssim 10^{10} {\rm cm}^{-3}$, never stops the
contraction. The structure of the contracting disk reaches that of a singular
solution as the density and the column density obey $\rho(r)\propto r^{-2}$ and
$\sigma(r) \propto r^{-1}$, respectively. The magnetic field strength on the
mid-plane is proportional to $\rho(r)^{1/2}$ and further that of the center
($B_c$) evolves as proportional to the square root of the gas density ($\propto
\rho_c^{1/2}$). It is shown that isothermal clouds experience ``run-away''
collapses. The evolution after the equation of state becomes hard is also
discussed.
