  On 2022 March 28 two successive coronal mass ejections (CMEs) were observed
by multiple spacecraft and resulted in a magnetic cloud (MC) at 1 AU. We
investigate the propagation and interaction properties of the two CMEs
correlated with the MC using coordinated multi-point remote sensing and in situ
observations from Solar Orbiter, STEREO A, SOHO, and Wind. The first CME was
triggered by a filament eruption with a high inclination angle. Roughly 9 hr
later, the second CME originating from the same active region erupted with a
smaller tilt angle and faster speed compared to the first one. The second CME
overtook the preceding CME and formed a merged front at approximately 75
\rsun{}, which developed into a complex ejecta at 1 AU. The descending speed
and low proton temperature inside the complex ejecta suggest that the two CMEs
have fully merged before reaching 1 AU, leading them to begin expanding rather
than compressing against each other. The complex ejecta appears to have the
magnetic field and plasma signatures of an MC, although there is a
discontinuity in the magnetic field implying previous interactions. The cross
section of the complex ejecta, reconstructed from in situ data using a
Grad-Shafranov technique, exhibits a right--handed flux rope structure. These
results highlight that an MC--like complex ejecta lacking interaction features
could arise from the complete merging of two CMEs.
