  For Gaussian initial conditions the perturbation theory predicts a very
specific hierarchy for the projected matter $p$-point correlation functions. In
the small angle approximation and assuming a power-law spectrum I derive the
exact expressions of the coefficients $s_p$ relating the averaged $p$-order
angular correlation function, $\omb_p$ to the second one, $\omb_p=s_p\
\omb_2^{p-1}$. These results are valid for any selection function, but for a
top-hat angular filter only. These coefficients are found to be significantly
higher than their 3D counterparts, $S_p=\xib_p/\xib_2^{p-1}$.
  For the coefficient $s_3$ I discussed the accuracy of the small angle
approximation by computing, for particular examples, its angular dependence
with Monte-Carlo numerical integrations. It is found that the accuracy of the
small angle approximation for $\theta\approx 1^o$ slightly depends on the
selection function. Using the selection function expected for galaxy catalogues
the approximation is found to be reasonably good.
  The measurements of the $s_p$ parameters made in the APM angular survey are
found to give systematic lower values than the theoretical predictions. How
significant this discrepancy is and what the implications would be for galaxy
formation models is discussed in the last section.
