Stars often form in multiple systems and may follow a complex evolution involving mass transfer and collisions, leading to mergers that are possible progenitors of Type Ia supernovae (SNe) [1, 2]. The progenitors of such explosions are still highly debated . While binaries have received much attention so far, higher-order stellar systems show a wide variety of interactions especially in tight systems, like long-term gravitational effects playing a key role in triple (where they are called von Zeipel-Lidov-Kozai , [4, 5], hereafter ZLK, oscillations) and quadruple systems. Here we report on the properties of the first spectroscopic quadruple (SB4) found within a star cluster: the 2+2 hierarchical system HD 74438 . Its membership in the open cluster IC 2391 makes it the youngest (43 My) SB4 discovered so far. The eccentricity of the 6 y outer period is 0.46 and the two inner orbits, with periods of 20.5 d and 4.4 d, and eccentricities of 0.36 and 0.15, are not coplanar. Using an innovative combination of ground-based high resolution spectroscopy [7, 8, 9, 10] and Gaia/Hipparcos astrometry [11, 12, 13, 14], we show that this system is undergoing secular interaction that likely pumped the eccentricity of one of the inner orbit higher than expected for the spectral types of its components. We compute the future evolution of HD 74438 by considering gravitational dynamics, stellar evolution, and binary interactions , and show that this system is an excellent candidate progenitor of sub-Chandrasekhar Type Ia supernova through white dwarf (WD) mergers. This specific type of SNIa better accounts for the chemical evolution of iron-peak elements in the Galaxy .