  We consider the evolution of a system containing a population of massive
planets formed rapidly through a fragmentation process occurring on a scale on
the order of 100 au and a lower mass planet that assembles in a disc on a much
longer timescale. During the formation phase, the inner planet is kept on a
circular orbit due to tidal interaction with the disc, while the outer planets
undergo dynamical relaxation. Interaction with the massive planets left in the
system after the inner planet forms may increase the eccentricity of the inner
orbit to high values, producing systems similar to those observed.
