  We report new results in our continuing study of the unique compact (1 pc
extent), nearby (d = 97 pc), young (t = 9 Myr) stellar cluster dominated by the
B9 star eta Chamaeleontis. An optical photometric survey spanning 1.3 x 1.3 pc
adds two M5-M5.5 weak-lined T Tauri (WTT) stars to the cluster inventory which
is likely to be significantly complete for primaries with masses > 0.15 M_sun.
The cluster now consists of 17 primaries and approximately 9 secondaries lying
within 100 AU of their primaries. The apparent distribution of 9:7:1
single:binary:triple systems shows 2-4 x higher multiplicity than in the field
main sequence stars, and is comparable to that seen in other pre-main sequence
(PMS) populations. The initial mass function (IMF) is consistent with that of
rich young clusters and field stars. By extending the cluster IMF to lower
masses, we predict 10-14 additional low mass stars with 0.08 < M < 0.15 M-sun
and 10-15 brown dwarfs with 0.025 < M < 0.08 M_sun remain to be discovered. The
eta Cha cluster extends the established stellar density and richness
relationship for young open clusters. The radial distribution of stars is
consistent with an isothermal sphere, but mass segregation is present with > 50
percent of the stellar mass residing in the inner 6 arcmin (0.17 pc).
Considering that the eta Cha cluster is sparse, diffuse and young, the cluster
may be an ideal laboratory for distinguishing between mass segregation that is
primordial in nature, or arising from dynamical interaction processes.
