We investigated the origin of the Planetary Nebula (PN) M 1-16 using narrow band optical imaging, and high and low resolution optical spectra to perform a detailed morphokinematic and chemical studies. M 1-16 is revealed to be a multipolar PN that predominantly emits in [O III] in the inner part of the nebula and [N II] in the lobes. A novel spectral unsharp masking technique was applied to the position-velocity maps (PVs) to reveal a set of multiple structures at the centre of M 1-16 spanning radial velocities from -40km/s to 20km/s, with respect to the systemic velocity . The morphokinematic model indicates that the deprojected velocity of the lobe outflows are >100km/s, and particularly the larger lobes and knots have a deprojected velocity of ~350km/s; the inner ellipsoidal component has a deprojected velocity of ~29km/s. A kinematical age of 8700yr has been obtained from the model assuming an homologous velocity expansion law and a distance of 6.2kpc. The chemical analysis indicates that M 1-16 is a Type I PN with a central star of PN (CSPN) mass in the range of ~0.618-0.713Msun and an initial mass for the progenitor star between 2.0 and 3.0Msun (depending on metalicity). An Teff~140000K and log(L/Lsun)=2.3 was estimated using the 3MdB photoionization models to reproduce the ionisation stage of the PN. All these results lead us to suggest that M 1-16 is an evolved PN, contrary to the scenario of proto-PN suggested in previous studies. We propose that the mechanism responsible for the morphology of M 1-16 is related to the binary (or multiple star) evolution scenario.