  The angular correlation function \wth of faint galaxies is affected both by
nonlinear gravitational evolution and by magnification bias due to
gravitational lensing. We compute the resulting \wth for different cosmological
models and show how its shape and redshift evolution depend on \Omega and
\Lambda. For galaxies at redshift greater than 1 (R magnitude fainter than
about 24), magnification bias can significantly enhance or suppress \wth,
depending on the slope of the number-magnitude relation. We show for example
how it changes the ratio of \wth for two galaxy samples with different
number-count slopes.
