  We have simulated the formation of large-scale structure arising from
COBE-normalized spectra computed by convolving a primordial double-inflation
perturbation spectrum with the CDM transfer function. Due to the broken scale
invariance ('BSI') characterizing the primordial perturbation spectrum, this
model has less small-scale power than the (COBE-normalized) standard CDM model.
The particle-mesh code (with $512^3$ cells and $256^3$ particles) includes a
model for thermodynamic evolution of baryons in addition to the usual
gravitational dynamics of dark matter. It provides an estimate of the local gas
temperature. In particular, our galaxy-finding procedure seeks peaks in the
distribution of gas that has cooled. It exploits the fact that ``cold"
particles trace visible matter better than average and thus provides a natural
biasing mechanism. The basic picture of large-scale structure formation in the
BSI model is the familiar hierarchical clustering scenario. We obtain particle
in cell statistics, the galaxy correlation function, the cluster abundance and
the cluster-cluster correlation function and statistics for large and small
scale velocity fields. We also report here on a semi-quantitative study of the
distribution of gas in different temperature ranges. Based on confrontation
with observations and comparison with standard CDM, we conclude that the BSI
scenario could represent a promising modification of the CDM picture capable of
describing many details of large-scale structure formation.
