  We investigate the dynamics of interstellar dust particles in moderately high
resolution ($512^3$ grid points) simulations of forced compressible transonic
turbulence including self-gravity of the gas. Turbulence is induced by
stochastic compressive forcing which is delta-correlated in time. By
considering the nearly Jeans-unstable case, where the scaling of the simulation
is such that a statistical steady state without any irreversible collapses is
obtained, we obtain a randomly varying potential, acting as a second stochastic
forcing. We show that, in this setting, low-inertia grains follow the gas flow
and cluster in much the same way as in a case of statistical steady-state
turbulence without self-gravity. Large, high-inertia grains, however, are
accelerated to much higher mean velocities in the presence of self-gravity.
Grains of intermediate size also show an increased degree of clustering. We
conclude that self-gravity effects can play an important role for
aggregation/coagulation of dust even in a turbulent system which is not
Jeans-unstable. In particular, the collision rate of large grains in the
interstellar medium can be much higher than predicted by previous work.
