  We study the interplay between mass transfer, accretion and gravitational
torques onto a black hole binary migrating in a self-gravitating, retrograde
circumbinary disc. A direct comparison with an identical prograde disc shows
that: (i) because of the absence of resonances, the cavity size is a factor
a(1+e) smaller for retrograde discs; (ii) nonetheless the shrinkage of a
circular binary semi--major axis, a, is identical in both cases; (iii) a
circular binary in a retrograde disc remains circular while eccentric binaries
grow more eccentric. For non-circular binaries, we measure the orbital decay
rates and the eccentricity growth rates to be exponential as long as the binary
orbits in the plane of its disc. Additionally, for these co-planar systems, we
find that interaction (~ non--zero torque) stems only from the cavity edge plus
a(1+e) in the disc, i.e. for dynamical purposes, the disc can be treated as a
annulus of small radial extent. We find that simple 'dust' models in which the
binary- disc interaction is purely gravitational can account for all main
numerical results, both for prograde and retrograde discs. Furthermore, we
discuss the possibility of an instability occurring for highly eccentric
binaries causing it to leave the disc plane, secularly tilt and converge to a
prograde system. Our results suggest that there are two stable configurations
for binaries in self-gravitating discs: the special circular retrograde case
and an eccentric (e~ 0.6) prograde configuration as a stable attractor.
