  We address the high peaks found by Steidel et al (1997) in the redshift
distribution of ``Lyman-break'' objects (LBOs) at redshift z~3. The highest
spike represents a relative overdensity of 2.6 in the distribution of LBOs in
pixels of comoving size ~10Mpc/h. We examine the likelihood of such a spike in
the redshift distribution within a suite of models for the evolution of
structure in the Universe, including models with Omega=1 (SCDM and CHDM) and
with Omega=0.4-0.5 (LCDM and OCDM). Using high-resolution dissipationless
N-body simulations, we analyze deep pencil-beam surveys from these models in
the same way that they are actually observed, identifying LBOs with the most
massive dark matter halos. We find that all the models (with SCDM as a marginal
exception) have a substantial probability of producing spikes similar to those
observed, because the massive halos are much more clumped than the underlying
matter -- i.e., they are biased. Therefore, the likelihood of such a spike is
not a good discriminator among these models. We find in these models that the
mean biasing parameter b of LBOs with respect to dark matter varies within a
range b ~2-5 on a scale of ~10Mpc/h. We also compute the two-body correlation
functions of LBOs predicted in these models. The LBO correlation functions are
less steep than galaxies today (gamma ~1.4), but show similar or slightly
longer correlation lengths.
