With more than one central mass, as in the situation where equal masses are co-orbiting the center of mass, there may exist situations where outside objects orbit the center of mass of another system that is orbiting its own center of mass.  In such a situation, the characteristic orbits can exist, however, if the orbital paths come too close to the orbits of the central masses, a gravitational difference which is complicated may disrupt the motion of the orbiting masses leading to chaotic results.

In this scene, m3-6 are set to orbit the c.o.m. of the two inner bodies in four characteristic ways.  Because of the close proximity of the elliptical orbit to the orbit of m1, however, the orbit is not altogether easily predictable:

As can be seen, the motion of the close to circular orbiting body is disturbed as well by the oscillation of the central bodies, and the elliptical orbit is greatly disturbed and will soon become irregular, and eventually it will be ejected from the system.

It is possible to have a system where 3 equal mass objects orbit each other, however, since it is impossible to have greater than 3 equidistant objects in 2-d space (the limit for 3-d space is 4), there is a theoretical limit of 3 objects orbiting a common center of mass with exactly the same motion (displaced by their angle distance from each other).