  (abridged)We use a sample of ~200,000 galaxies drawn from the Sloan Digital
Sky Survey to study how clustering depends on properties such as stellar mass
(M*), colour (g-r), 4000A break strength (D4000), concentration index (C), and
stellar surface mass density (\mu_*). We find that more massive galaxies
cluster more strongly than less massive galaxies, with the difference
increasing above the characteristic stellar mass of the Schechter mass
function. When divided by physical quantities, galaxies with redder colours,
larger D4000, higher C and larger \mu_* cluster more strongly. The clustering
differences are largest on small scales and for low mass galaxies. At fixed
stellar mass,the dependences of clustering on colour and 4000A break strength
are similar. Different results are obtained when galaxies are split by
concentration or surface density. The dependence of w(r_p) on g-r and D4000
extends out to physical scales that are significantly larger than those of
individual dark matter haloes (> 5 Mpc/h). This large-scale clustering
dependence is not seen for the parameters C or \mu_*. On small scales (< 1
Mpc/h), the amplitude of the correlation function is constant for ``young''
galaxies with 1.1 < D4000< 1.5 and a steeply rising function of age for
``older'' galaxies with D4000>1.5. In contrast, the dependence of the amplitude
of w(r_p) on concentration on scales less than 1 Mpc/h is strongest for
disk-dominated galaxies with C<2.6. This demonstrates that different processes
are required to explain environmental trends in the structure and in star
formation history of galaxies.
