  We investigate the roles of magnetically driven disk wind (MDW) and thermally
driven photoevaporative wind (PEW) in the long-time evolution of protoplanetary
disks. We start simulations from the early phase in which the disk mass is
$0.118\,{\mathrm{M}_{\odot}}$ around a $1\,{\mathrm{M}_{\odot}}$ star and track
the evolution until the disk is completely dispersed. We incorporate the mass
loss by PEW and the mass loss and magnetic braking (wind torque) by MDW, in
addition to the viscous accretion, viscous heating, and stellar irradiation. We
find that MDW and PEW respectively have different roles: magnetically driven
wind ejects materials from an inner disk in the early phase, whereas
photoevaporation has a dominant role in the late phase in the outer
($\gtrsim1\,$au) disk. The disk lifetime, which depends on the combination of
MDW, PEW, and viscous accretion, shows a large variation of $\sim1$-$20\,$Myr;
the gas is dispersed mainly by the MDW and the PEW in the cases with a low
viscosity and the lifetime is sensitive to the mass-loss rate and torque of the
MDW, whereas the lifetime is insensitive to these parameters when the viscosity
is high. Even in disks with very weak turbulence, the cooperation of MDW and
PEW enables the disk dispersal within a few Myr.
