  A basic ingredient to understand large scale fluctuations in our present day
Universe is the initial conditions. Using N-body simulations, we compare the
clustering that arises from Gaussian and non-Gaussian initial conditions. The
latter is motivated by a global texture model which has initial $J$-order
correlations $\xibar_J$ close to the strongly non-Gaussian regime $\xibar_J
\simeq \xibar_2^{J/2}$. The final amplitudes $S_J \equiv
\xibar_J/\xibar_2^{J-1}$ in the non-Gaussian (texture) model evolves slowly
towards the (Gaussian) gravitational predictions but, even at $\sigma_8=1$, are
still significantly larger, showing a characteristic minimum with a sharp
increase in $S_J$ with increasing scales. This minimum, which is between $10$
and $15 \Mpc$, depending on the normalization, separates the regime where
gravity starts dominating the evolution from the one in which the initial
conditions are the dominant effect. In comparing this results with galaxy
clustering observations, one has to take into account {\it biasing}, i.e. how
galaxy fluctuations trace matter fluctuations. Although biasing could change
the amplitudes, we show that the possible distortions to the shape of $S_J$ are
typically small. In contrast to the non-Gaussian (texture) predictions, we find
no significant minimum or rise in $S_J$ obtained from the APM Galaxy Survey.
