  Hierarchical massive quadruple systems are ideal laboratories for examining
the theories of star formation, dynamical evolution, and stellar evolution. The
successive mergers of hierarchical quadruple systems might explain the mass gap
between neutron stars and black holes. Looking for light curves of O-type
binaries identified by LAMOST, we find a (2+2) quadruple system: TYC
3340-2437-1, located in the stellar bow-shock nebula (SBN). It has a
probability of over 99.99\% being a quadruple system derived from the surface
density of the vicinity stars. Its inner orbital periods are 3.390602(89) days
and 2.4378(16) days, respectively, and the total mass is about (11.47 + 5.79) +
(5.2 + 2.02) = 24.48 $M_{\odot}$. The line-of-sight inclinations of the inner
binaries, B$_1$ and B$_2$, are 55.94 and 78.2 degrees, respectively, indicating
that they are not co-planar. Based on observations spanning 34 months and the
significance of the astrometric excess noise ($D>2$) in Gaia DR3 data, we guess
that its outer orbital period might be a few years. If it were true, the
quadruple system might form through the disk fragmentation mechanism with outer
eccentric greater than zero. This eccentricity could be the cause of both the
arc-like feature of the SBN and the noncoplanarity of the inner orbit. The
outer orbital period and outer eccentric could be determined with the release
of future epoch astrometric data of Gaia.
