  Standard inflation with one scalar field produces primordial perturbations
with a nearly flat ('Harrison-Zeldovich') power spectrum. Here we consider
first, a double inflation spectrum, and second, a massive scalar field with an
interaction potential which mimics an early quartic interaction, but fading
away at a characteristic scale. We solve numerically the linear perturbation
equations with initial conditions due to scalar field quantum fluctuations at
the initial horizon crossing. The resulting power spectra are shown to be
non-flat, exhibiting either a break or a valley. Using the transfer function of
cold dark matter model we study the influence of the shape of primordial power
spectra on observations of large scale structure in the universe. We compare
the power spectra in redshift space with reconstructed power spectra from the
IRAS catalogue. Further we discuss the variances of galaxy counts in cells, and
the mass function of galaxy clusters. Comparison with standard CDM demonstrates
the advantages and benefits of the more complicated initial spectra.
