  We explore the clustering of galaxy groups in the Galaxy and Mass Assembly
(GAMA) survey to investigate the dependence of group bias and profile on
separation scale and group mass. Due to the inherent uncertainty in estimating
the group selection function, and hence the group auto-correlation function, we
instead measure the projected galaxy--group cross-correlation function. We find
that the group profile has a strong dependence on scale and group mass on
scales $r_\bot \lesssim 1 h^{-1} \mathrm{Mpc}$. We also find evidence that the
most massive groups live in extended, overdense, structures. In the first
application of marked clustering statistics to groups, we find that group-mass
marked clustering peaks on scales comparable to the typical group radius of
$r_\bot \approx 0.5 h^{-1} \mathrm{Mpc}$. While massive galaxies are associated
with massive groups, the marked statistics show no indication of galaxy mass
segregation within groups. We show similar results from the IllustrisTNG
simulations and the L-Galaxies model, although L-Galaxies shows an enhanced
bias and galaxy mass dependence on small scales.
