The planetary nebula LMC-N66 is an extraordinary object, as it is the only confirmed PN where the central star is a Wolf-Rayet star of type [WN]. Moreover, the star showed a dramatic brightness outburst in 1993-1994. In a previous papers we analyzed the changing stellar spectra and found evidence that the central star is most likely a binary system where a white dwarf presently accretes matter from a non-degenerate companion at a high rate. Thus the object is a candidate for a future type Ia supernova in our cosmic neighborhood. We have also analyzed the morphology and kinematics of the nebula, using images and high-resolution spectra obtained with the HST. The object presents a complex multipolar structure, dominated by very bright lobes located at both sides of the central star and separated by a narrow waist. In addition there is a pair of very extended and twisted loops, also pointing in opposite directions; their symmetry axis and collimation angle differs from those of the bright lobes. High resolution spectroscopy reveals two main velocity components, "approaching" material at an average systemic radial velocity of V = -50 km/s and similarly bright "receding" material at V= 50 km/s. Opposite lobes and loops possess opposite velocities. Furthermore there are knots and filaments of complex structure and kinematics. The morphology and kinematics of LMC-N66 can be explained as the result of episodic bipolar ejections with changing axis. The bipolar structures could have been produced by collimated streams ejected from a precessing central source. The precession could have been produced by an external torque, possibly due to a binary companion.