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We have generated surface-brightness projections of large-scale structure simulations (at different epochs) in the Einstein and ROSAT bandpasses in order to calculate the probabilities of misidentifying filaments and projected groups as rich clusters. Cluster masses are tracked as a function of time in order to estimate cluster merger and mass accretion rates. We also show how cluster profiles vary with time and fit King models to the cold, hot and baryonic components in order to estimate core radii and slopes. The particular simulations used for this analysis self-consistently evolve both baryons (gas) and dark matter in a CHDM universe. The X-ray properties of the resulting clusters have already been shown to agree well with observational results(Bryan et. al 1994).
