The simulated matter distribution on large scales is studied using core-sampling , cluster analysis , inertia tensor analysis , and minimal spanning tree techniques .
Seven simulations in large boxes for five cosmological models with COBE normalized CDM-like power spectra are studied .
The wall-like Super Large Scale Structure with parameters similar to the observed one is found for the OCDM and \Lambda CDM models with \Omega _ { m } h = 0.3 ~ { } \&~ { } 0.245 .
In these simulations , the rich structure elements with a typical value for the largest extension of \sim ( 30 - 50 ) h ^ { -1 } Mpc incorporate \sim 40 % of matter with overdensity of about 10 above the mean .
These rich elements are formed due to the anisotropic nonlinear compression of sheets with original size of \sim ( 15 - 25 ) h ^ { -1 } Mpc .
They surround low-density regions with a typical diameter \sim ( 50 - 70 ) h ^ { -1 } Mpc .

The statistical characteristics of these structures are found to be approximately consistent with observations and theoretical expectations .
The cosmological models with higher matter density \Omega _ { m } = 1 in CDM with Harrison-Zeldovich or tilted power spectra can not reproduce the characteristics of the observed galaxy distribution due to the very strong disruption of the rich structure elements .
Another model with a broken scale invariant initial power spectrum ( BCDM ) shows not enough matter concentration in the rich structure elements .