  We estimate the rate at which the proposed space gravitational-wave
interferometer LISA could detect intermediate-mass black-hole binaries, that
is, binaries containing a black hole in the mass range 10 -- 100 Msun orbiting
a black hole in the mass range 100 -- 1000 Msun. For one-year integrations
leading up to the innermost stable orbit, and a signal-to-noise ratio of 10, we
estimate a detection rate of only 1 per million years for 10 Msun/100 Msun
binaries. The estimate uses the method of parameter estimation via matched
filtering, incorporates a noise curve for LISA established by the LISA Science
Team that is available online, and employs an IMBH formation rate model used by
Miller (2002). We find that the detectable distance is relatively insensitive
to LISA arm lengths or acceleration noise, but is roughly inversely
proportional to LISA position errors, and varies roughly as T^(1/2), where T is
the integration time in years. We also show that, while all IMBH systems in
this mass range may be detected in the Virgo cluster up to 40 years before
merger, none can be detected there earlier than 400 years before merger. An
extended LISA mission that enabled 10-year integrations could detect IMBH
systems at the Virgo cluster 1000 years before merger, and systems in galactic
globular clusters a million years before merger. We compare and contrast these
estimates with earlier estimates by Miller (2002).
