  We examine the implications of Modified Newtonian Dynamics (MOND) on the
large scale structure in a Friedmann-Robertson-Walker universe. We employ a
``Jeans swindle'' to write a MOND-type relationship between the fluctuations in
the density and the gravitational force, $\vg$. In linear Newtonian theory,
$|\vg|$ decreases with time and eventually becomes $<g_0$, the threshold below
which MOND is dominant. If the Newtonian initial density field has a power-law
power-spectrum of index $n<-1$, then MOND domination proceeds from small to
large scale. At early times MOND tends to drive the density power-spectrum
towards $k^{-1}$, independent of its shape in the Newtonian regime. We use
N-body simulations to solve the MOND equations of motion starting from initial
conditions with a CDM power-spectrum. MOND with the standard value $g_0=10^{-8}
cm s^{-2}$, yields a high clustering amplitude that can match the observed
galaxy distribution only with strong (anti-) biasing. A value of $g_0 \approx
10^{-9}cm s^{-2}$, however, gives results similar to Newtonian dynamics and can
be consistent with the observed large scale structure.
