  The Kepler-1647 is a binary system with two Sun-type stars (approximately
1.22 and 0.97 Solar mass). It has the most massive circumbinary planet (1.52
Jupiter mass) with the longest orbital period (1,107.6 days) detected by the
Kepler probe and is located within the habitable zone (HZ) of the system. In
this work, we investigated the ability to form and house an Earth-sized planet
within its HZ. First, we computed the limits of its HZ and performed numerical
stability tests within that region. We found that HZ has three sub-regions that
show stability, one internal, one co-orbital, and external to the host planet
Kepler-1647b. Within the limits of these three regions, we performed numerical
simulations of planetary formation. In the regions inner and outer to the
planet, we used two different density profiles to explore different conditions
of formation. In the co-orbital region, we used eight different values of total
disc mass. We showed that many resonances are located within regions causing
much of the disc material to be ejected before a planet is formed. Thus, the
system might have two asteroid belts with Kirkwood gaps, similar to the Solar
System\'s main belt of asteroids. The co-orbital region proved to be extremely
sensitive, not allowing the planet formation, but showing that this binary
system has the capacity to have Trojan bodies. Finally, we looked for regions
of stability for an Earth-sized moon. We found that there is stability for a
moon with this mass up to 0.4 Hill\'s radius from the host planet.
