  I outline the connections between some of the most widely used statistical
measures of galaxy clustering and the fundamental issues in the theory of
structure formation. I devote particular attention to the problem of biasing,
i.e. to a possible difference between the distribution of galaxies and the
distribution of mass. Using numerical experiments, I show that a local
morphology-density relation leads to different slopes and amplitudes for the
correlation functions of different galaxy types on small scales, but that the
correlation functions on large scales all have the same shape, differing only
by constant factors. I also examine a variety of biasing models in which the
efficiency of galaxy formation depends on local properties of the mass
distribution. While these purely local influences do lead to a large-scale
bias, in all cases the bias factor becomes constant on scales larger than the
galaxy correlation length.
