  We explore, using numerical simulations, the influence of mass and distance
on the evolution of triple black hole systems. Following in the direction of
Burrau's famous 3,4,5 problem, black holes are initially placed at the vertices
of Pythagorean triangles. Numerical integration of orbits was conducted using
relativistic corrections (post-Newtonian) up to the 2.5$^{th}$ order with
ARCcode. As a descriptor of the evolution of the systems, the lifetimes, the
number of two-body encounters and the number of mergers were all analysed. We
found that as the mass unit of the black holes increased there was strong
positive correlation with the fraction of mergers (0.9868), strong negative
correlation with the average number of two-body encounters (-0.9016) and the
average lifetimes of the triple systems decayed exponentially (determination
coefficient of 0.9986). Around the mass unit range of
10$^{5.5}$M$_{\odot}$-10$^{5.6}$M$_{\odot}$, there was a transition from escape
dominated dynamics to merger dominated dynamics. However, in the mass unit
range of 10$^6$ M$_{\odot}$ $-$ 10$^{9}$M$_{\odot}$ with 1 pc distance unit, we
find that 25\% of cases resulted in the escape of a supermassive black hole
(SMBH) which may be a cause for wandering SMBH's found in some
galaxies/galactic merger remnants.
