  The currently standard theory of cosmic structure formation posits that the
present-day clumpy appearance of the universe developed through gravitational
amplification of the matter density fluctuations that are generated in the very
early universe. The energy content of the univese and the basic statistics of
the initial density field have been determined with a reasonable accuracy from
recent observations of the cosmic microwave background, large-scale structure,
and distant supernovae. It has become possible to make accurate predictions
from the standard model. We review the latest observations and the recent
progress in the theory of structure formation at low and high redshifts. Two
promising methods to probe large-scale matter distribution are introduced and
the future prospects are discussed. Results from state-of-the-art cosmological
simulations are also presented.
