  In this article, we compare the properties of two coronal mass ejections
(CMEs) that show similar source region characteristics but different
evolutionary behavior in the later phases. We discuss the two events in terms
of their near-Sun characteristics, interplanetary evolution, and
geo-effectiveness. We carefully analyzed the initiation and propagation
parameters of these events to establish the precise CME-ICME connection and
their near-Earth consequences. The First event was associated with poor
geo-magentic storm disturbance index (Dst $\approx$-20 nT) while the second
event is associated with intense geomagnetic storm of DST $\approx$-119 nT. The
configuration of the sunspots in the active regions and their evolution are
observed by Helioseismic and Magnetic Imager (HMI). For source region imaging,
we rely on data obtained from Atmospheric Imaging Assembly (AIA) on board Solar
Dynamics Observatory (SDO) and H$\alpha$ filtergrams from Solar Tower Telescope
at Aryabhatta Research Institute of Observational Sciences (ARIES). For both
the CMEs, flux rope eruptions from the source region triggered flares of
similar intensities ($\approx$M1). At the solar source region of the eruptions,
we observed circular ribbon flare (CRF) for both the cases, suggesting
fan-spine magnetic configuration in the active region corona.
