  We present narrow-, broad-band, and WISE archive images, and high- and
intermediate-resolution long-slit spectra of K 4-37, a planetary nebula that
has never been analyzed in detail. Although K 4-37 appears bipolar, the
morphokinematical analysis discloses the existence of three distinct axes and
additional particular directions in the object, indicating that K 4-37 is a
multi-axis planetary nebula that has probably been shaped by several bipolar
outflows at different directions. A 4-6 M$_{\odot}$ main-sequence progenitor is
estimated from the derived high nebular He and N abundances, and very high N/O
abundance ratio ($\sim$2.32). The general properties are compatible with K 4-37
being a highly evolved planetary nebula located at $\sim$14 kpc. The WISE image
at 22 $\mu$m reveals K 4-37 to be surrounded by a large ($\sim$13$\times$8
pc$^2$) elliptical detached shell probably related to material ejected from the
AGB progenitor. The observed elliptical morphology suggests deformation of an
originally spherical AGB shell by the ISM magnetic field or by the influence of
a companion. We compare K 4-37 and NGC 6309 and found remarkable similarities
in their physical structure but noticeably different chemical abundances that
indicate very different progenitor mass. This strongly suggests that,
irrespective of the initial mass, their (presumably binary) central stars have
shared a very similar mass ejection history.
