  We consider a cosmological model with non-Gaussian initial perturbations,
which in principle could be generated in non-standard inflationary scenarios
with two or more scalar fields. In particular we focus our attention on the
model proposed by Linde & Mukhanov (1997) perturbations are quadratic in a
Gaussian field. These perturbations, if they exist, have to be observable as a
non-Gaussian distribution of the CMB signal on the sky. In order to efficiently
pick up the non-Gaussian signal in CMB maps of degree resolution, one can use
Minkowski Functionals and peak statistics. Our paper contains the theoretical
predictions of the properties for Minkowski Functionals and distributions of
peaks of the CMB anisotropy in the model with "squared" Gaussian statistics.
Likelihood comparison of the four-year COBE DMR data to this non-Gaussian model
and the standard Gaussian model does not select any of them as most likely. We
also suggest an efficient algorithm for fast simulation of CMB maps on the
whole sky. Using a cylindrical partition of the sphere, we rewrite the
spherical harmonics analysis as a Fourier transform in flat space, which makes
the problem accessible to numerically advantageous FFT methods.
