  The evolution of protostellar outflow is investigated with resistive
magneto-hydrodynamic nested-grid simulations that cover a wide range of spatial
scales (\sim 1AU - 1pc). We follow cloud evolution from the pre-stellar core
stage until the infalling envelope dissipates long after the protostar
formation. We also calculate protostellar evolution to derive protostellar
luminosity with time-dependent mass accretion through a circumstellar disk. The
protostellar outflow is driven by the first core prior to protostar formation
and is directly driven by the circumstellar disk after protostar formation. The
opening angle of the outflow is large in the Class 0 stage. A large fraction of
the cloud mass is ejected in this stage, which reduces the star formation
efficiency to \sim 50%. After the outflow breaks out from the natal cloud, the
outflow collimation is gradually improved in the Class I stage. The head of the
outflow travels more than \sim 10^5AU in \sim 10^5 yr. The outflow momentum,
energy and mass derived in our calculations agree well with observations. In
addition, our simulations show the same correlations among outflow momentum
flux, protostellar luminosity and envelope mass as those in observations. These
correlations differ between Class 0 and I stages, which is explained by
different evolutionary stages of the outflow; in the Class 0 stage, the outflow
is powered by the accreting mass and acquires its momentum from the infalling
envelope; in the Class I stage, the outflow enters the momentum-driven
snow-plough phase. Our results suggest that protostellar outflow should
determine the final stellar mass and significantly affect the early evolution
of low-mass protostars.
