  We estimate the two-point correlation function of dark matter haloes, with
masses >10^{13} h^{-1} Mo, that have or not significant substructure. The
haloes are identified with a friends of friends algorithm in a large LCDM
simulation at two redshift snapshots (z=0 and 1), while halo substructure is
determined using an observationally driven method. We find in both epochs a
clear and significant signal by which haloes with substructure are more
clustered than those with no-substructure. This is true for all the considered
halo mass ranges, although for the highest halo masses the signal is noisy and
present only out to ~20 h^{-1} Mpc. There is also a smooth increase of the halo
correlation length with increasing amplitude of the halo substructure. We also
find that substructured haloes are typically located in high-density
large-scale environments, while the opposite is true for non-substructured
haloes. If the haloes found in high-density regions have a relatively earlier
formation time, as suggested by recent works, then they do indeed have more
time to cluster than haloes, of a similar mass, which form later in the
low-density regions. In such a case one would have naively expected that the
former (earlier formed) haloes would typically be dynamically more relaxed than
the latter (later formed). However, the higher merging and interaction
rate,expected in high-density regions, could disrupt their relatively relaxed
dynamical state and thus be the cause for the higher fraction of haloes with
substructure found in such regions.
