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It is likely that most protostellar systems undergo a brief phase where theprotostellar disc is self-gravitating. If these discs are prone tofragmentation, then they are able to rapidly form objects that are initially ofseveral Jupiter masses and larger. The fate of these disc fragments (and thefate of planetary bodies formed afterwards via core accretion) dependssensitively not only on the fragment's interaction with the disc, but with itsneighbouring fragments.  We return to and revise our population synthesis model of self-gravitatingdisc fragmentation and tidal downsizing. Amongst other improvements, the modelnow directly incorporates fragment-fragment interactions while the disc isstill present. We find that fragment-fragment scattering dominates the orbitalevolution, even when we enforce rapid migration and inefficient gap formation.  Compared to our previous model, we see a small increase in the number ofterrestrial-type objects being formed, although their survival under tidalevolution is at best unclear. We also see evidence for disrupted fragments withevolved grain populations - this is circumstantial evidence for the formationof planetesimal belts, a phenomenon not seen in runs where fragment-fragmentinteractions are ignored.  In spite of intense dynamical evolution, our population is dominated bymassive giant planets and brown dwarfs at large semimajor axis, which directimaging surveys should, but only rarely, detect. Finally, disc fragmentation isshown to be an efficient manufacturer of free floating planetary mass objects,and the typical multiplicity of systems formed via gravitational instabilitywill be low.

Towards a population synthesis model of self-gravitating disc fragmentation and tidal downsizing II: The effect of fragment-fragment interactions